DES16C3cje: A low-luminosity, long-lived supernova
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DES16C3cje : A low-luminosity, long-lived supernova. / Gutierrez, C. P.; Sullivan, M.; Martinez, L.; Bersten, M. C.; Inserra, C.; Smith, M.; Anderson, J. P.; Pan, Y-C; Pastorello, A.; Galbany, L.; Nugent, P.; Angus, C. R.; Barbarino, C.; Carollo, D.; Chen, T-W; Davis, T. M.; Della Valle, M.; Foley, R. J.; Fraser, M.; Frohmaier, C.; Gonzalez-Gaitan, S.; Gromadzki, M.; Kankare, E.; Kokotanekova, R.; Kollmeier, J.; Lewis, G. F.; Magee, M. R.; Maguire, K.; Moller, A.; Morrell, N.; Nicholl, M.; Pursiainen, M.; Sollerman, J.; Sommer, N. E.; Swann, E.; Tucker, B. E.; Wiseman, P.; Aguena, M.; Allam, S.; Avila, S.; Bertin, E.; Brooks, D.; Buckley-Geer, E.; Burke, D. L.; Rosell, A. Carnero; Kind, M. Carrasco; Carretero, J.; Costanzi, M.; da Costa, L. N.; De Vicente, J.; DES Collaboration.
In: Monthly Notices of the Royal Astronomical Society, Vol. 496, No. 1, 25.05.2020, p. 95-110.Research output: Contribution to journal › Journal article › Research › peer-review
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TY - JOUR
T1 - DES16C3cje
T2 - A low-luminosity, long-lived supernova
AU - Gutierrez, C. P.
AU - Sullivan, M.
AU - Martinez, L.
AU - Bersten, M. C.
AU - Inserra, C.
AU - Smith, M.
AU - Anderson, J. P.
AU - Pan, Y-C
AU - Pastorello, A.
AU - Galbany, L.
AU - Nugent, P.
AU - Angus, C. R.
AU - Barbarino, C.
AU - Carollo, D.
AU - Chen, T-W
AU - Davis, T. M.
AU - Della Valle, M.
AU - Foley, R. J.
AU - Fraser, M.
AU - Frohmaier, C.
AU - Gonzalez-Gaitan, S.
AU - Gromadzki, M.
AU - Kankare, E.
AU - Kokotanekova, R.
AU - Kollmeier, J.
AU - Lewis, G. F.
AU - Magee, M. R.
AU - Maguire, K.
AU - Moller, A.
AU - Morrell, N.
AU - Nicholl, M.
AU - Pursiainen, M.
AU - Sollerman, J.
AU - Sommer, N. E.
AU - Swann, E.
AU - Tucker, B. E.
AU - Wiseman, P.
AU - Aguena, M.
AU - Allam, S.
AU - Avila, S.
AU - Bertin, E.
AU - Brooks, D.
AU - Buckley-Geer, E.
AU - Burke, D. L.
AU - Rosell, A. Carnero
AU - Kind, M. Carrasco
AU - Carretero, J.
AU - Costanzi, M.
AU - da Costa, L. N.
AU - De Vicente, J.
AU - DES Collaboration
PY - 2020/5/25
Y1 - 2020/5/25
N2 - We present DES16C3cje, a low-luminosity, long-lived type II supernova (SN II) at redshift 0.0618, detected by the Dark Energy Survey (DES). DES16C3cje is a unique SN. The spectra are characterized by extremely narrow photospheric lines corresponding to very low expansion velocities of less than or similar to 1500 km s(-1), and the light curve shows an initial peak that fades after 50 d before slowly rebrightening over a further 100 d to reach an absolute brightness of M-r similar to 15.5 mag. The decline rate of the late-time light curve is then slower than that expected from the powering by radioactive decay of Co-56, but is comparable to that expected from accretion power. Comparing the bolometric light curve with hydrodynamical models, we find that DES16C3cje can be explained by either (i) a low explosion energy (0.11 foe) and relatively large Ni-56 production of 0.075 M-circle dot from an similar to 15 M-circle dot red supergiant progenitor typical of other SNe II, or (ii) a relatively compact similar to 40 M-circle dot star, explosion energy of 1 foe, and 0.08 M-circle dot of Ni-56. Both scenarios require additional energy input to explain the late-time light curve, which is consistent with fallback accretion at a rate of similar to 0.5 x 10(-)(8) M-circle dot s(-1).
AB - We present DES16C3cje, a low-luminosity, long-lived type II supernova (SN II) at redshift 0.0618, detected by the Dark Energy Survey (DES). DES16C3cje is a unique SN. The spectra are characterized by extremely narrow photospheric lines corresponding to very low expansion velocities of less than or similar to 1500 km s(-1), and the light curve shows an initial peak that fades after 50 d before slowly rebrightening over a further 100 d to reach an absolute brightness of M-r similar to 15.5 mag. The decline rate of the late-time light curve is then slower than that expected from the powering by radioactive decay of Co-56, but is comparable to that expected from accretion power. Comparing the bolometric light curve with hydrodynamical models, we find that DES16C3cje can be explained by either (i) a low explosion energy (0.11 foe) and relatively large Ni-56 production of 0.075 M-circle dot from an similar to 15 M-circle dot red supergiant progenitor typical of other SNe II, or (ii) a relatively compact similar to 40 M-circle dot star, explosion energy of 1 foe, and 0.08 M-circle dot of Ni-56. Both scenarios require additional energy input to explain the late-time light curve, which is consistent with fallback accretion at a rate of similar to 0.5 x 10(-)(8) M-circle dot s(-1).
KW - supernovae: general
KW - supernovae: individual: (DES16C3cje)
KW - TIDAL DISRUPTION
KW - PAIR-INSTABILITY
KW - STAR-FORMATION
KW - LIGHT CURVES
KW - LATE TIMES
KW - SN 2005CS
KW - EVOLUTION
KW - FALLBACK
KW - TRANSIENTS
KW - PHOTOMETRY
U2 - 10.1093/mnras/staa1452
DO - 10.1093/mnras/staa1452
M3 - Journal article
VL - 496
SP - 95
EP - 110
JO - Royal Astronomical Society. Monthly Notices
JF - Royal Astronomical Society. Monthly Notices
SN - 0035-8711
IS - 1
ER -
ID: 271540713